This submission converts our ACS corongraphy program to NICMOS coronagraphy in the F110W filter. The program fits in its original allocation of 9 orbits, and has the same observing strategy: a three-orbit block visit to each target, consisting of 2 orbits on the science target at roll angles separated by ~25 degrees, followed by a 1 orbit observation of a PSF standard. New visit numbers 11-19 were created to replace ACS visits 1-9 (which should be withdrawn). Due to the poorer coronagraphic perfomance of NICMOS relaive to ACS, one of our science targets has been changed. HD 38858 and its PSF star HD 33093 have been replaced by HR 506 and its PSF star HD 7570. The disk of HD 38858 was right at the performance limit of the ACS coronagraph, and is unlikely to be detected with NICMOS (whose contrast rejection is 3x worse than what the ACS coronagraph provided). The replacement target, HR 506, has a disk 4x dustier than that of HD 38858 - giving us a much better chance at detection - and has also been detected by us with ACS in our Cycle 14 program. Please implement visits 14-19 immediately for flight, as these observations were approved for transfer from ACS to NICMOS on the original program targets. Visits 11-13 should be on-hold pending the outcome of the PCR regarding the change to targret HR 506 and its PSF star. ----- Submission 1 (Fri May 05 17:00:26 GMT 2006) ----- ----- Attempting Submission 2 (Tue Jun 19 22:19:44 GMT 2007) ----- Assigned ID: 365 ----- Submission 1 (Fri Jan 27 19:51:37 GMT 2006) ----- Coronagraphic Imaging of Bright New Spitzer Debris Disks II. Fifteen percent of bright main sequence stars possess dusty circumstellar debris disks revealed by far-infrared photometry. These disks are signposts of planetary systems: collisions among larger, unseen parent bodies maintain the observed dust population against losses to radiation pressure and P-R drag. Images of debris disks at optical, infrared, and millimeter wavelengths have shown central holes, rings, radial gaps, warps, and azimuthal asymmetries which indicate the presence of planetary mass perturbers. Such images provide unique insights into the structure and dynamics of exoplanetary systems. Relatively few debris disks have been spatially resolved. Only thirteen have ever been resolved at any wavelength, and at wavelengths < 10 microns (where subarcsec resolution is available), only ten. Imaging of many other debris disk targets has been attempted with various HST cameras/coronagraphs and adaptive optics, but without success. The key property which renders a debris disk observable in scattered light is its dust optical depth. The ten disks imaged so far all have a dust excess luminosity >~ 0.01% that of the central star; no disks with smaller optical depths have been detected. Most main sequence stars known to meet this requirement have already been observed, so future progress in debris disk imaging depends on discovering additional stars with large infrared excess. The Spitzer Space Telescope offers the best opportunity in 20 years to identify new examples of high optical depth debris disk systems. We propose to complete ACS coronagraphic imaging followup of bright, new debris disks discovered during the first two years of the Spitzer mission, by observing three additional targets in Cycle 15. Our goal is to obtain the first resolved images of these disks at ~3 AU resolution, define the disk sizes and orientations,and uncover disk substructures indicative of planetary perturbations. The results will open wider a window into the structure of planetary systems.
A star having a suspected circumstellar disk will be observed on the ACS/HRC. In the first orbit, a short exposure in F606W will be taken without the coronagraph to provide photometry (the star will be somewhat saturated). Then, a coronagraphic acquisition exposure is taken, followed by a long coronagraphic exposure in F606W. Between the first and second orbit the telescope is rolled 20-30 degrees. In the second orbit, an acquisition and long coronagraphic exposure is taken. The telescope is then slewed to a reference PSF star. In this third orbit, a short F606W exposure is taken, followed by acquisition and long F606W coronagraphic exposures. 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